text:
Babar Wiki
Babar and the Adventures of Badou
Ghost for a Day
Babar: The Movie
Tale of Two Siblings
The Celesteville Enquirer
Remember When...?
Babar's First Step
Badou
Alan Templeton & Mary Crawford
The Show Must Go On is the 10th episode of season 1 as well as the 10th episode overall
While the Triplets are putting on a show and Julian is being difficult. Babar tells the children when he once dealt with a difficult prima ballerina, Mademoiselle Soretoza.
At the school auditorium, the triplets are practicing the play "Rapunzel" with their friends. Julian however does not like the name Rapunzel, even saying, "Either the name goes or I go!" They take a break and Flora tells Babar that Julian won't listen. Babar tells her that the show must go on, no matter how difficult a performer is. Babar tells them about the time he worked with someone very difficult as well, the greatest ballerina in the world, Mademoiselle Soretoza.
Back when Babar was younger, he asked her to come to Celesteville to perform, however this took a lot of persuading to get her to come, but she eventually agrees. When she arrives, she throws her cape onto Pompadour, Babar welcomes her and introduces her to Celeste who will be her understudy. She very gracefully greets them but throws the bouquet Celeste gave her into Pompadour's face and goes upstairs to get some sleep. With the rehearsals beginning tomorrow, Celeste is honored to be dancing with her. That night, the Mademoiselle had a difficult time sleeping, she complained about her bed, Chef Truffles's meal, and the Spring Waters. They were starting to realize that she was not going to be easy to please. Babar is happy that all the shows were sold out, telling Pompadour this will be a great show. Suddenly there is a shout coming from the Mademoiselle's dressing room, Babar comes in and finds her head buried in a sandbox and won't come out until Babar deals with the director. They won't see eye to eye and the Mademoiselle declares that either he leaves or she does, fed up the director quits right on the spot. Babar becomes worried who will take his place, the Mademoiselle tells Babar he is more than capable of being the director, as long as he follows her directions. Cornelius and Pompadour see if Babar is all right and he tells them he is now the show's director.
Over the next few days, rehearsals were in progress, but with all of the Mademoiselle's outbursts, many of the company had already left and Babar was stuck in the middle. Even when the make-up person made a small mistake, the Mademoiselle sends her away. Meanwhile, word has spread to Rhinoland about Mademoiselle Soretoza's performance. Lady Rataxes was a big fan of hers and asks Rataxes to attend with her, but he prefers fencing over ballet. She tells him that if he does see a ballet performance, he would be known for having some culture, and it would do him justice. While hesitant at first, he agrees as to not let his wife believe she married a barbarian. Back in Celesteville, with time running out, rehearsals were in full swing, even though half the company was gone. Lord and Lady Rataxes along with Basil attend the rehearsal, the Mademoiselle is pleased to have a fan of hers in her presence. Babar tries to tell Lady Rataxes that these are closed rehearsals, but the Mademoiselle asks Babar to make an exception for a "patron of the arts," he agrees. Lady Rataxes is enjoying the show, but Lord Rataxes is bored. Meanwhile, a blue spotlight appears over Mademoiselle Soretoza which makes her scream. Babar says he'll ask the lighting man to change it, but she says they should just change the lighting man, as a sign of him quitting, the lighting man dims the lights, one at a time, much to Celeste's dismay.
With the days wearing on, everyone's patience is growing thin. The slightest offense caused her to go to her dressing room causing the rehearsals to be put on hold. He asks Celeste to fill in for the Mademoiselle, when she shows the Mademoiselle how hard she has been working, the Mademoiselle insults Celeste by telling Babar not to waste his time, saying if she herself can't make it, there is no show. This hurts Celeste's feelings to the point where she runs offstage crying. Babar is starting to get fed up with the Mademoiselle for how she is treating others. Cornelius tells Babar that the show must go on, but Babar says that at the rate the Mademoiselle is going, there won't be a show.
Babar goes to check on a brokenhearted Celeste, and he finds her crying backstage. He comfortingly tells her that she is a wonderful dancer, but Celeste feels that it isn't good enough for the Mademoiselle. Babar assures her that no matter what the Madamoiselle says, she should ignore her. Celeste stops crying, but Babar tells her is ready to cancel the show. Celeste tells Babar that they are working so hard and that the audience is looking forward to the show. She therefore promises that she'll practice harder if Babar lets the show proceed. Hugging her with his trunk, Babar accepts the deal. After a rehearsal, they decide to run it again from the top, but before they start, Rataxes snores very loudly which annoys Lady Rataxes.
With only three days left until the show, the remaining cast and crew practiced at every opportunity, then one day, the inevitable happens. A small mistake happens, as the conductor apparently miscues her, and the leading man Felipe fails to catch her, and she blames the conductor and Felipe, even insulting them to the point where they quit. She even tells off Lord Rataxes for his snoring, this deeply hurts Lady Rataxes who leaves to go and stay with her mother. The show now has absolutely no cast or crew aside from Babar, the Mademoiselle and Celeste. Babar wishes they had something to help and Celeste then tells Babar that they have their friends and staff, this gives Babar an idea. Basil tells Babar that Rataxes wants the show to go on, Babar tells Basil the show will go on.
The day before the premier, Babar calls everyone to the theatre for an emergency meeting, they are all going to put on the show themselves, they all have some theatre experience and talent themselves. Pompadour will do the lighting since he helped pick out the chandeliers for the palace, Zephir will do the curtain and backdrop, Cornelius, who once filled in as a conductor for a marching band, will be in charge of the orchestra, Madame will take care of the costumes, Arthur would be in charge of the props and Celeste will dance for the Mademoiselle and fill in as make-up person. Rataxes has an idea of who could be the leading man, Babar says they'll deal with that later. They start practicing and there are some troubles during rehearsal, from Cornelius losing his baton, to Arthur and Zephir having troubles with the sets, to Celeste having trouble getting into character. After a night's worth of rehearsals, they were able make it through a successful run through, and were ready for the premiere that night. All they needed was a leading man for the performance. They were all proud of their achievement and are ready.
That night, everyone was arriving, but there is no sign of the leading lady, Zephir tells Babar to come with him. Lady Rataxes is worried that she would be humiliated by her husband. Backstage, Babar tells her that everything is ready but the Mademoiselle won't work with any of them simply for being amateurs (compared to those they are replacing). Babar insists that they have been working very hard and there won't be a show without them. She tells Babar that she is the show and that she will perform solo. Babar, now officially fed up with her attitude and insults, not only refuses this idea, but tells her off. She leaves and everyone is proud of Babar for standing up to her. He says that they will perform the show without her. Instead, they have Celeste replacing her as the leading lady, and Babar says that Rataxes is their leading man. Like they are to have a leading man, he is desperate to win his wife's heart back.
During the show, Babar becomes worried when he doesn't hear a sound from the audience, he looks out and after Rataxes catches Celeste, the audience roars. They all bow and the show is a complete success.
Celeste recalls Rataxes was able to dance so well, thanks to his fencing skills, which he had always prided himself on. Julian, who overheard the story, comes out and says to forget about changing the name Rapunzel. Flora is thrilled to hear that and calls places. Celeste says that this will be a great show even without Rataxes. The rehearsal goes on well.
Lord Rataxes
Lady Rataxes
Mademoiselle Soretoza (only appearance)
Julian (only appearance)
Other girl as Rapunzel (only appearance)
In this episode, we find out Celeste took ballet.
This episode is based on one of Babar's books.
Lady Rataxes is a big fan of ballet and even tells Rataxes the people like a cultured king.
The book version reveals the lion conductor's name to be Leon.
Julian does not appear in the book version. Instead, it is Alexander who plays the prince there.
It is never mentioned who was playing Rapunzel in the show, but it must have been a friend of Flora's
A plothole in a future episode had many fans wondering, in "All Played Out," Celeste says that she has dreamed about being on the stage since she was little, but she performs in this episode, she may have forgotten about the events.
The scene where the paper hanger hangs the signs of the countdown to the performance is recycled.
Lord and Lady Rataxes wouldn't have been able to get tickets at the point of their appearance as the show was already sold out.
More Babar Wiki
1 Babar
2 Celeste
3 Cornelius
Babar Wiki is a FANDOM TV Community.


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Family/Educational
City Concerts
Virtual & Live Streaming
Harmony Artists
The best source for musical, theatrical, and special event entertainment nationwide
Corporate Events/Talent Buying Services
Artist The Everly Set
The Everly Set
The Everly Set– Acclaimed singer-songwriters Sean Altman (founder Rockapella) and Jack Skuller (Disney Recording Artist) present the ultimate concert celebration of the legendary Everly Brothers. The Everly Set whisks your audience to 1957 when teens Phil and Don Everly first supercharged the sound of Rock'n'Roll with the sparkling harmonies that influenced The Beatles, Simon & Garfunkel, The Beach Boys, The Bee Gees, and The Eagles. With hits like Bye Bye Love, Wake Up Little Susie, Cathy's Clown, All I Have To Do Is Dream, and When Will I Be Loved; and Everly versions of hits by Merle Haggard, The Beatles, Buddy Holly, and Simon & Garfunkel, The Everly Set's vocals and keen wit will have your audience singing, laughing, and dancing in the aisles! Available as a duo or quartet.
Video Samples at THEEVERLYSET.COM
(c) 2020 HarmonyArtists.com

redpajama_set_name: RedPajamaCommonCrawl


Sesmie Global is currently hiring warehouse workers to help complete shipments by processing and loading orders.
Prepares orders by processing requests and supply orders, pulling materials, packing boxes, placing orders in delivery area.
Maintains truck or van by completing preventive maintenance requirements, arranging for repairs.
Maintains safe and clean work environment by keeping shelves, pallet area, and workstations neat, maintaining clean shipping supply area, complying with procedures, rules, and regulations.
Maintains technical knowledge by attending educational workshops, reviewing publications.
Previous work experience as a warehouse worker.


Although you may think of awkward metal wires and misery when someone suggests straightening your teeth, today's orthodontists provide braces for kids and adults that can correct your smile without embarrassment. If you usually shy away from the idea of braces, you should check out options like discreet ceramic braces or invisible aligner trays. The many benefits of realigning your smile are worth the investment.
Straight teeth are easier to brush and floss, so straightening your smile can have a positive impact on your oral health. Getting braces as an adult can reduce your risk of gum disease and tooth decay. If you have a misaligned bite or jaw pain, braces can be an important part of treating those conditions. Having a straighter smile can influence how others see you. A study of people's reactions to photos of individuals with both straight and crooked teeth showed that people with straight teeth got higher ratings on such attributes as leadership ability, popularity, and even athletic ability.
Even if you had braces as a kid, your teeth can shift as you age. The length of time adults need to wear braces varies, since it can take longer for adult teeth to move into position than children's. The duration of most treatments ranges from one to three years. Once your teeth are correctly aligned you will likely need to wear a retainer. Your orthodontist can attach permanent retainers to the backs of your teeth.
The cost of orthodontics varies significantly by treatment type, but a good dental plan can cover all or part of orthodontic treatment, making affordable braces a reality. You may be eligible for a discount if you can pay the entire fee up front. If you can't, talk to your orthodontist about a payment plan.


text:
namespace BackTesting.Model.Portfolio
{
    using System;
    using System.Collections.Generic;
    using BackTesting.Model.Events;

    public interface IPortfolio
    {
        void UpdateSignal(SignalEvent signal);
        void UpdateFill(FillEvent fill);
        void UpdateTimeIndex(MarketEvent market);
        IDictionary<DateTime, Holding> HoldingHistory { get; }
        IDictionary<DateTime, decimal> GetEquityCurve();
    }
}

redpajama_set_name: RedPajamaGithub


Produce an attention-grabbing video to attract customers and sales leads. Preparing for a trade show booth and a trade show video production can be a daunting task for many customers. To "wow" the trade show and convention visitors is of particular importance. Ideally, you'd like the video's effect to last long after the trade show or convention is over. Therefore, here are several key points which will help your organization instruct your video production team to produce a captivating four-minute loop for trade show video booth.
The Western Massachusetts region is quite fortunate to be the home of many fabulous filmmakers and videographers. This post takes a look at some of the video production services Western Mass companies and organizations provide.


text:
27-9 CAS Shanghai converts syngas aerosols to medium- and long-chain chemicals using Clostridium ljungdahlii
by rsc | Sep 27, 2021 | News
A group around Weihong JIANG at CAS Institute of Plant Sciences in Shanghai metabolically engineered autotrophic Clostridium ljungdahlii to efficiently co-produce three important bulk chemicals, isopropanol, 3-hydroxybutyrate (3-HB), and ethanol (together, IHE), using syngas (CO2/CO). The engineered strain was further optimized to reassimilate acetic acid and synthesize 3-HB by introducing heterologous functional genes. Finally, the best-performing strain was able to produce 13.4, 3.0, and 28.4 g/L of isopropanol, 3-HB, and ethanol, respectively, in continuous gas fermentation.
https://doi.org/10.1021/acssynbio.1c00235
© CAS Institute of Plant Sciences, Shanghai


text:
\section{Introduction} \label{sec:intro}

Daily observations of the white-light solar corona with the Large Angle and Coronal Spectrometer (LASCO) aboard the Solar and Heliospheric Observatory (SoHO) allowed to discover more than three thousands comets plunging into the harsh solar atmosphere \citep{Battams2017}. Because of the proximity of their perihelion, such comets are usually referred to as sungrazers. \citet{Jones2018} gave a more tight classification of comets based on their perihelion distance ($q$) and distinguished between near-sun comets ($q<66.1~\mathrm{R}_\odot$ from the centre of the Sun), sunskirting ($3.45~\mathrm{R}_\odot <q<33.1~\mathrm{R}_\odot$), sungrazing ($q=1.0-3.45~\mathrm{R}_\odot$), and sundiving ($q<1.0~\mathrm{R}_\odot$) comets. Based on their orbits, sungrazing comets are grouped into families since they are fragments of a common progenitor, like, the Kreutz group. Commonly, sungrazing comets appear in coronagraphs as small and fast-moving bright dots with a short tail, but some of them are outstanding events, with very long tails and bright comas. When approaching the Sun, the majority of these comets are completely dissolved within a couple of solar radii from the Sun's surface. Nevertheless, two comets were observed in the FoV of the Atmospheric Imaging Assembly (AIA) of the Solar Dynamics Observatory (SDO), hence at distances below 0.7 $\mathrm{R}_\odot$ from the solar surface in the extreme ultra-violet wavelengths (EUV): comets C/2011 N3 \citep{Schrijver2012} and C/2011 W3 (Lovejoy) \citep{Downs13}. Another comet approaching the Sun in November 2013, C/2012 S1 (ISON), disregarded expectations and failed to show EUV signatures of its passage in the corona, probably because of the lower size of its nucleus that could not withstand the intense heat from the Sun \citep{Bryans2016}.

The transit of Comet Lovejoy in December 2011 was exceptional. The comet crossed the corona from East to  West, with the perihelion located behind the Sun as observed from Earth, at only $\sim0.2~\mathrm{R}_\odot$ from the Sun's surface. The images recorded by SDO in the different EUV channels of AIA showed a trail of striations, also referred to as {\it striae}. \citet{Bryans2012} associated the EUV striae to the temporal evolution of the excited states of oxygen ions released by the comet nucleus and guided along the local magnetic field lines, which were emitting in EUV as a consequence of the increase in their relative abundance. \citet{Downs13} used sophisticated MHD simulations to reproduce the observations and provided estimates of the magnetic field and coronal density of the corona.
\citet{McCauley2013} focused on the post-perihelion observations of Lovejoy from AIA and included in their analysis X-Ray Telescope (XRT) data from Hinode. They determined the ionisation stages in the observed striae and determined other physical parameters, such as the out-gassing rate of the nucleus and the mass of the comet. \citet{Raymond2014} also analysed the striae left by the comet during the outbound phase, estimated the speed of propagation and broadening of the striae along the local magnetic field, and used an MHD model and the theory of pick-up ions to compare the measurements with theoretical expectations.
They found that cometary ions outline flux tubes with diameters of about 4000 km and that density variations between neighbouring flux tubes reach at least a factor of six on a scale of few thousand kilometers. The measurements were compared with an MHD model and the theory of pick up ions to show that part of the energy of the cometary ions as they isotropize  goes to Alfv\'en waves. However, \citet{Raymond2014} did not consider the Coulomb interaction between oxygen ions and the background coronal plasma when estimating velocities and densities.

In general, the relevance of comets relies on the possibility to exploit them as natural probes of the inner heliosphere and solar corona. In fact, even before the advent of exploration by spacecraft, the direction of plasma tails of comets observed from Earth during their transit was thought as an evidence of solar wind flow \citep{1951ZA.....29..274B,1958ApJ...128..664P}. Several studies on comet observations aimed at determining the physical condition of the interplanetary medium (solar wind speed, density, temperature etc.) and assessing the physical processes at work in the coupling between the solar wind and comet tails \citep{2007ApJ...668L..79V,2015ApJ...812..108D,2018A&A...615A.143N}. Along the same lines, sungrazing comets have been used to infer the conditions of the solar corona but at distances much further from the photosphere, using the SoHO/LASCO and UVCS instruments \citep{2007P&SS...55.1021B, 2018ApJ...858...19R}. In the case of Comet Lovejoy,
the importance in studying the EUV striae concerns the possibility to diagnose the physical conditions of the low solar corona at distances inaccessible to spacecraft. Even Parker Solar Probe, which will attain a minimum distance of 9.8 $\mathrm{R}_\odot$, will also not be able to get as close to the solar surface as Comet Lovejoy did.

In this work, we aim at studying the time evolution of the striae by modeling the propagation of oxygen ions along a magnetic flux tube. The length of a stria is determined by the ion beam velocity, which decays because of collisions, and the ion collisional diffusion. By determining the parameters characterizing the beam slowing down and the collisional dispersion, we can get estimates of the ambient plasma density at the location where the striae are formed.
The paper is organised as follows: in Section \ref{sec:obs} we present the observations of Lovejoy from SDO/AIA; in Section \ref{sec:modeling} we show how the striae of Comet Lovejoy are modeled; Section \ref{sec:analysis} discusses the analysis of the SDO/AIA data and the comparison with the numerical modeling. Finally, the discussion and conclusions are given in Section \ref{sec:disc}.

\section{Observations} \label{sec:obs}

\begin{figure}[htpb]
    \centering

        \includegraphics[width=1.0\textwidth]{figure1.png}

    \caption{Left panels: Composite images taken at different times with SDO/AIA in the 171 channel and showing the tail of striae left by Comet Lovejoy enclosed within two continuous red lines before (top panels) and after (bottom) the transit at the perihelion. The orbit of the comet is shown as a dotted red line. Right panels: blow-up view of the regions where striae are formed. The corresponding regions are outlined with a dashed red box in the left panels. The filled green circles labelled by letters mark the locations where intensity profiles are extracted and plotted in Fig. \ref{fig:int_vs_cpos}.}
    \label{fig:context_image}
\end{figure}

The perihelion transit of Comet Lovejoy was seen by different space observatories. SDO/AIA recorded the approach to the perihelion between 23:25 and 00:16 UT on December 15--16, 2011. For that occasion, the pointing axis of SDO/AIA was offset by about half degree to observe the comet entering in the corona. Afterward, the comet was seen to re-emerge from the perihelion on the West side between 00:40 and about 01:00 UT.
Fig. \ref{fig:context_image} shows a composite image taken in the 171 \AA~ channel of SDO/AIA showing the inbound (top panels) and outbound phases of the comet (bottom panels). The images in the top panels are processed with the Noise Adaptive Fuzzy Equalization tron (NAFE) algorithm \citep{2013ApJS..207...25D}.
The trajectory of the comet is superimposed onto the images as a dashed red line and is computed with SPICE: the SPICE kernel file was downloaded from the Horizons System \footnote{\url{https://ssd.jpl.nasa.gov/horizons/app.html\#/}} and read with the routines of the Spiceypy Python package \citep{Annex2020}. FITS file images were download from the JSOC service and read using the \texttt{read\_sdo.pro} routine in SolarSoftWare (SSW)/IDL.
We did not process the FITS files with the standard routine \texttt{aia\_prep.pro} because the images of the sequence were not correctly calibrated based on the FITS header information. The images were taken with a 12-second cadence (which was almost uniform during the observations) and a pixel size $\Delta_{\mathrm{pix}}\approx$0.56$"$. Some persistent jitter in the inbound phase data was removed by co-aligning each image of the sequence to the middle one taken at 23:51:36.58 UT.
As shown in Fig. \ref{fig:context_image}, the passage of the comet inside the solar corona left a trail of EUV striae. The striae appeared a minute after the transit of the comet nucleus. In Fig. \ref{fig:int_vs_cpos} we show the intensity profiles versus time extracted from six different locations along the projected path followed by the comet. In each panel, the vertical dashed red line marks the time instant when the comet nucleus passed through the point, the dotted black line indicates the time when the EUV intensity starts to increase. Indeed, the stria signature is found as an increase, more or less sharp, in the EUV intensity. The time-lag varies between 8--9 minutes. These time-lags have to be corrected for the light travel time from the Sun to the Earth, which is about 8 min. After correction, the definitive time-lag between the passage of the comet and the appearance of an EUV stria is within at most one minute, thus confirming the estimate provided in \citet{McCauley2013} in different EUV bands.
The striae appear different in length and brightness, reflecting the amount of emitting oxygen ions, which in turn depend on the local density of the corona. In the next Section we explain how the striae of Comet Lovejoy are modeled, in order to calculate intensity profiles and compare them with those obtained from the observations.

\begin{figure}
    \centering
        \includegraphics[width=1.0\textwidth]{intensity_vs_position.png}
    \caption{Intensity profiles vs. time taken at six different locations along the path of the comet. The dashed red line marks the time instant of the transit of the comet nucleus. The vertical dotted line indicates the moment at which the EUV emission starts to increase, hence when the oxygen ions starts to emit. The time lag is calculated between these two vertical lines and must be corrected for the light travel time to the observer.}
    \label{fig:int_vs_cpos}
\end{figure}

\section{Modeling of EUV Striae}\label{sec:modeling}

\subsection{Theoretical model}

\begin{figure}[htpb]
    \centering
    \includegraphics[width=.8\textwidth]{cartoon.pdf}
    \caption{Scheme of the mechanism for the formation of the striae}
    \label{fig:fig1}
\end{figure}

Following \citet{Downs13}, we assume that the cometary material is extracted from the comet during its travel through the solar corona, and that this material is rapidly ionized.
Once oxygen and other atoms are ionized, they are captured by the magnetic field and start to spiral around the straight field lines, moving along them with a velocity $u_0$ that can be estimated as the projection of the ion velocity along the magnetic field, $u_0 = {\bf v}_i\cdot{\bf B}/B$. A schematic representation is reported in Fig. \ref{fig:fig1}. The initial ion velocity can be seen as the sum of the comet velocity ${\bf v}_c$, and the ion outflow velocity ${\bf v}_{out}$, which is usually modeled as radial with respect to the comet nucleus \citep{Bryans2012}: ${\bf v}_i = {\bf v}_c + {\bf v}_{out}$.

As time goes on, oxygen ions reach higher ionization levels until they emit in the 171 \AA~line and are detected by SDO/AIA. This happens mainly for the ionization states O$^{4+}$ and O$^{5+}$ \citep{Downs13,Pesnell14} and implies that oxygen ions will be visible in 171 \AA~only some time after the comet passage, as discussed in the previous section. Later, these ions will be further ionized to O$^{6+}$ and more (e.g., by photioniosation, charge exchange, electron and proton collisions), so that emission in the 171 \AA~line fades out. In the meanwhile, oxygen ions move along the magnetic field and slow down because of collisions. They are also undergoing a diffusive spreading because of their disordered motion, due to the outflow velocity ${\bf v}_{out}$ and to collisions \citep[][Supplementary Material]{Downs13}.

The cloud of oxygen ions is spreading in the corona in three dimensions, however, since the Larmor radius is only a few km, which is much smaller than the striae length, we limit ourselves to a one dimensional modeling with the $x$ direction along the magnetic field, also  considering that (i) the spreading along the line-of-sight can be taken into account by integrating along the line of sight, something which is implicit in the EUV observations; and (ii) the spreading in the plane-of-sky and perpendicular to the $x$ direction is taken into account by actually summing the EUV signal over 4--5 pixels in that direction (see Section \ref{sec:analysis}), which also allows to improve the signal-to-noise ratio.

Therefore, we propose a simple modeling of the beam of oxygen ions, which are treated as test-particles.  The initial velocity along the mean field direction decreases because of collisions as
\begin{equation}
u(t) = u_0 e^{-t/\tau_{\rm slow}} \, ,
\end{equation}
where $\tau_{\rm slow}$ is the time for the collisional slowing down of a suprathermal ion beam in a field plasma (see below).
We consider that ${\bf v}_{out}$ is symmetric, $<{\bf v}_{out}>=0$, and that for the beam $u_0$ is given by the average of ${\bf v}_i$, so that $u_0 = {\bf v}_c \cdot {\bf B}/B$. Then, the position of the beam head $x_0(t)$ is
\begin{equation}
x_0(t) = x_{00} + u_0 \tau_{\rm slow}\left[1-\exp(-t/\tau_{\rm slow})\right]
\label{eq_beam}
\end{equation}
where $x_{00}$ is the starting position of the beam, just after the release of ionized material from the comet into the solar corona. The above expression shows that, basically, the length of a stria is given by $u_0 \tau_{\rm slow}$, to which the spreading due to collisional diffusion has to be added. Here, we study the distribution of material along the magnetic field by a probabilistic description taking into account both the beam \lq\lq ordered\rq\rq motion and the ion diffusive spreading. By using a methodology adopted for the transport of energetic particles accelerated at shock waves \citep{Ragot97,Perri08,Zim18}, we model the number density $n(x,t)$ of ions along the magnetic field as
\begin{equation}
        n(x,t) =  \int_0^t dt' \int_{-\infty}^{+\infty} dx' Q(x',t',t) P(x-x', t-t')
\label{eq_density}
\end{equation}
where the source of oxygen ions is given by
\begin{equation}
        Q(x',t',t) =   \eta(t)\Phi(t') \delta(x'- x_0(t')) \, ,
\end{equation}
and $P(x-x', t-t')$ is the probability of observing a particle in $(x,t)$ if it was emitted in $(x',t')$.
Here, $Q(x',t',t)$ represents the number of ions emitted in the position $x'$ at time $t'$. The motion of the beam is given by $x_0(t')$, i.e., by Eq. \eqref{eq_beam}, and the delta function implies that the source is located at $x'=x_0(t')$. Further, $\Phi(t')$ models the ion injection from the comet; if injection were sharp and punctual, this could be modeled as $\delta(t'-t_0)$ \citep[see, e.g.,][]{leRoux19}. However, here we have to take into account that the emission of oxygen ions from the comet is a multi-step process that includes solid particles and dust leaving the comet; molecule sublimation and ionization; and then oxygen ions reaching the ionization states O$^{4+}$ and O$^{5+}$. These steps require a time of several tens of seconds, as evidenced by the time lags shown in Figure \ref{fig:int_vs_cpos}, also depending on the coronal density and on the size of the dust grains, and cannot be well described by a sharp injection. Instead, we model the ion injection as a Gaussian function delayed in time by $t_0$:
\begin{equation}
\Phi(t') = \frac{\Phi_0}{\sqrt{2\pi} {\sigma_{t_0}}} \exp\left[ -\frac{(t'-t_0)^2}{2\sigma_{t_0}^2}\right] \, .
\end{equation}
In other words, $t_0$ represents the average time for oxygen ions to reach the O$^{4+}$ and O$^{5+}$ states, after the comet transit, and $\sigma_{t_0}$ the typical half-duration of the injection process. It would be possible to consider an injection process which is not point-like but also spreads out in space. We reserve this for future work.

In addition, we introduce in $Q(x',t',t)$ a factor $\eta(t)$ which is not strictly related to ion injection, but rather is a decay factor which corresponds to the ion beam ageing. Here, $\eta(t)$ describes the fact that after some time the oxygen ions pass from O$^{5+}$ to O$^{6+}$ and therefore the emission in the line {171 \AA} becomes negligible. Keeping a certain analogy with energetic particle transport, this effect is often modeled as a loss term in the transport equation, i.e., $\partial f/\partial t \simeq -f/\tau_{L} $ with $f$ the particle distribution function and with $\tau_{L}$ the loss time \citep[e.g.,][]{Perri16,leRoux19}. Such a loss term leads to an exponential decay. Therefore, we model this factor as $\eta(t)= \exp(-t/\tau_{L})$, with $\tau_{L}$ the ion lifetime which is obtained from \citet{Pesnell14}, see below.

The probability $P(x-x', t-t')$ is given by the Gaussian propagator, which is appropriate in the case of collisional diffusion:
\begin{equation}
        P(x-x', t-t') =  \frac{1}{\sqrt{4\pi D_{xx}(t-t')}} \exp{\left[ -\frac{(x-x')^2}{4 D_{xx} (t-t')} \right]}
\label{eq_propag}
\end{equation}
where the diffusion coefficient along the $x$ direction is given by $D_{xx} = \frac{1}{3}v_{\rm ran}^2\tau_D$. Here, $v_{\rm ran}$ is the disordered ion velocity after the ion \lq\lq first\rq\rq collision, and $\tau_D$ the dispersion collision time (see discussion below).
We note that the oxygen ion beam represents a strongly non-thermal distribution which can be unstable, so that wave-particle interaction can also contribute to the ion slowing down and diffusive spreading \citep[e.g.,][]{Raymond2014}. Here, however, we overlook this possibility and concentrate on collisional effects.
By integrating Eq. \eqref{eq_density} over $x'$ and exploiting the delta function, we obtain
\begin{equation}
        n(x,t) =  \eta(t) \int_0^t dt' \Phi(t') \frac{1}{\sqrt{4\pi D_{xx}(t-t')}} \exp\left\{-\frac{\left[ x - u_0\tau_{\rm slow}(1-\exp(-t'/\tau_{\rm slow}))\right]^2}{4D_{xx}(t-t')}\right\}.
        \label{eq:eq_density_final}
\end{equation}
Further numerical integration over $t'$ gives the density profiles which can be used for comparison with the striae observations.

\subsection{Collision times for oxygen ions and model parameters}

The above modeling of the oxygen O$^{4+}$ and O$^{5+}$ density along the striae depends on a number of parameters. Keeping in mind that several simplifications are needed in order to obtain a manageable treatment, these parameters are determined as follows.

The initial beam speed along the magnetic field $u_0$ is obtained from the projection of the comet speed on the magnetic field direction; because of projection effects, the angle $\theta$ between $\bf B$ and ${\bf v}_c$ is not well known. We note that \citet{Downs13} consider that $u_0$ may be in the range 100--200 km s$^{-1}$, while \citet{Raymond2014} estimate a velocity parallel to the magnetic field of 183 km s$^{-1}$ for some striae during the egress of comet Lovejoy. Here, we consider similar values of $u_0$, of the order of $u_0=100$ km s$^{-1}$, which are determined also with the help of the observed motion of the stria front.
We consider that the ion outflow velocity, assumed to spring radially out of the comet, can also cause a significant spread in the value of $u_0$.

The temporal evolution of various ion fractional abundances has been studied by \citet{Pesnell14}; for O$^{4+}$ and O$^{5+}$, which give rise to the emission lines O$_{ V}$ and O$_{ VI}$, they find for an electron density $n_e = 10^7$ cm$^{-3}$ a rise time of about 50 and 200 s, respectively for O$^{4+}$ and O$^{5+}$, and an exponential decay time of 300 and 800 s, respectively. Since both ion species contribute to the {171 \AA}  emission line, considering that each oxygen ion goes through successive ionization states,  we assume a lifetime for UV emission of $\tau_L \simeq 10^3$ seconds, i.e., roughly the sum of the decay times for O$^{4+}$ and O$^{5+}$. On the other hand, the rise times reported by \citet{Pesnell14} and the time lags inferred from Figure \ref{fig:int_vs_cpos} are used to model the temporal evolution of emitting ion injection, that is, the delay time $t_0$ after the comet transit and the typical half-duration of the injection process: we assume initial values of $t_0 = 60$ s and $\sigma_{t_0} = 80$ s, and then adjust these values to best match each stria profile (see Table \ref{tab:tab2}).

For the elongation and spreading of the oxygen ion beam, basic parameters are the collision times $\tau_{\rm slow}$  and $\tau_D$, see Eqs. \eqref{eq_beam} and \eqref{eq_propag}.
Because of the nature of Coulomb collisions, which implies a cross-section decreasing as $U^{-4}$, with $U$ the relative speed between colliding particles \citep[e.g.,][]{2005ipp..book.....G}, the time $\tau_{\rm slow}$  for the slowing down of a suprathermal ion beam and the time $\tau_D$ for dispersion of suprathermal particles are longer than the collision time of thermal particles  \citep[e.g.,][]{Krall,Downs13}.
In turn, the suprathermal ions thermalize with the ambient plasma on a longer time scale than $\tau_{\rm slow}$ and $\tau_D$ \citep{Krall}. In this case, for an ion beam whose velocity is larger than the ion thermal velocity but slower than the electron thermal velocity, the following expression can be used \citep{Krall,Downs13}
\begin{equation}
\tau_{\rm slow} \approx \frac{{m_T}^2}{4\pi n_e e^2 {q_T}^2 \left[ \displaystyle{ \left(1+\frac{m_T}{m_p}\right)\frac{1}{U^3}+\frac{4}{3\sqrt{\pi}}\left(1+\frac{m_T}{m_e}\right) \left(\frac{m_e}{2\kappa T_e} \right)^{3/2} } \right]\ln\Lambda} \, ,
\label{eq:tau_slow}
\end{equation}
 with $m_T$ and $q_T$ the mass and charge of the suprathermal beam particles, $U$ the speed of suprathermal  particles, $e$  the elementary charge, $m_p$ and $m_e$ the masses of proton and electron, $\kappa$ the Boltzmann's constant, $\ln\Lambda \simeq 22$ the Coulomb's logarithm. We have also assumed a coronal electron temperature $T_e \sim 1.5$ MK. An initial ion speed of the order of $U\simeq v_c\simeq 500$ km s$^{-1}$ could be taken. Actually, when computing the density of each stria we considered the comet speed $v_c$ when it created the stria at a certain distance from the Sun $r_c$. We note that $U$ is assumed to correspond to the comet's speed because this is the initial ion speed which is involved in the collision processes, even if the average beam speed along the magnetic field $u_0$ is lower. In other words, we assume that gyromotion is not modifying the collision time since the gyroradius is very much larger than the inter-particle distance.
This collision time depends on the electron density $n_e$, which is kept as a free parameter to be determined by the fit of the observed emission profiles.

Now, we consider that after the first collision the ions of the beam move in random direction, that is, are subject to a diffusive motion. In such a scenario, we can assume that
the random velocity of dispersive motion $v_{\rm ran}$ decays exponentially from the initial speed of the ions $\sim v_c$ to the thermal speed of oxygen, $v_{th O}\simeq 40$ km s$^{-1}$. Here we assume an intermediate value $v_{\rm ran} = 150$ km s$^{-1}$, which is close to the geometrical mean of $v_c$ and $v_{th O}$; indeed, the geometrical mean, rather than the arithmetic mean, represents the fact that in an exponential decay the initial velocity quickly decreases.
Then, $\tau_D$ is determined by fitting the observed emission profiles in the EUV.
Indeed, even the dispersion time depends on the local density as \citep{Krall}
\begin{equation}
\tau_D \approx \frac{m_T^2 v_{\rm ran}^3}{16\pi n_e e^2 q_T^2 \ln\Lambda} \, ,
\label{eq:tau_d}
\end{equation}
so that determining $D_{xx} = \frac{1}{3}v_{\rm ran}^2\tau_D$ by fitting the observed brightness profiles, we are able to estimate $\tau_D$ and then $n_e$.

\begin{table}[htpb]
	\centering
	\begin{tabular}{l l}
	\hline
	{\bf Function or parameter} & {\bf Description} \\
	\hline
	\hline
	$\eta(t)=\eta_0 \exp(-t/\tau_{L})$ & Ion beam ageing \\
	$\tau_{L}$ & Ion lifetime \\
	$\Phi(t') = \frac{\Phi_0}{\sqrt{2\pi}\sigma_{t_0}} \exp\left[ -\frac{(t'-t_0)^2}{2\sigma_{t_0}^2}\right]$ & Ion flux injection\\
	$\tau_\mathrm{slow}$ &  Decay time of the beam\\
	$t_0$ & Injection time \\
	$\sigma_{t_0}$ & Time interval for ion injection \\
	$x(t') = x_{00} + u_0 \tau_\mathrm{slow}\left[1-\exp(-t'/\tau_\mathrm{slow})\right]$ & Motion of the beam \\
	$u_0$ &  Beam speed along the magnetic field\\
	$D_{xx} = \frac{1}{3}v_{\rm ran}^2\tau_D$ & Diffusion coefficient\\
	$v_{\rm ran}$ & Random speed of suprathermal ions\\
	$\tau_D$ & Diffusion time \\
	\hline
	\hline
	\end{tabular}
	\caption{Description of the functions and model parameters.}
	\label{tab:tab1}
\end{table}

\section{Data analysis and comparison with modeling} \label{sec:analysis}
\subsection{Striae intensity profiles from observations}

To study the temporal evolution of some of the striae observed in 171 \AA, we re-mapped the image data-set into a new 2D grid, having the same pixel size of the original images and with the horizontal axis ($x'$) parallel to the direction of motion of the comet and the vertical one ($y'$) strictly perpendicular to its trajectory. Such a perspective is shown in Fig. \ref{fig:remap_slits}. The comet path is outlined with a dotted red line and located at $y'=100$ pix in the top panel and $y'=150$ pix in the bottom panel. Online animations are also available.
Re-mapping is necessary to trace the striae in the corona. We noticed that the locations where the striae emission starts during the inbound phase of the comet does not lie perfectly on the dashed red line, which outlines the comet path, but it is shifted few pixels outwards. This is probably due to a systematic error in the position of the Sun's centre reported in the header of the FITS files when SDO/AIA was in off-pointing mode of observations. A physical explanation could also be found in the action of radiation pressure that pushes outwards the fragments and dust grains, before getting sublimated and ionised. However, this effect should be negligible in the present observations. In fact, such a shift is not evident in the outbound observations when SDO/AIA did return to pointing the Sun centre.
We manually selected few bright striae, which are marked by dashed blue lines and labelled as S1,..., S6 in Fig. \ref{fig:remap_slits}. The intensity extracted from each slit and averaged over a width of 11 pixels for all the available time steps is stacked into columns forming then a time-distance (TD) map (Fig. \ref{fig:tdmap_slits}). Time is on the horizontal axis, given in minutes with respect to the time $t_c$ when the comet passes through the slit. Distance on the vertical axis, measured with respect to the position where the comet crosses the slit, is given in units of 10$^3$ km.

\begin{figure}[htpb]
    \centering
    \includegraphics[width=1.0\textwidth]{figure4.png}
    \caption{Re-interpolated image of the transit of Comet Lovejoy during the inbound phase as seen from SDO/AIA in 171 \AA. The image is a composition of base ratio frames taken in the time interval indicated at the top of the panel. The red dashed line marks the comet path. The analysed striae are marked by the dashed blue lines, and labelled as S1--S3. The associated animation is available (inbound.mp4). The six seconds video covers the transit of Comet Lovejoy in the corona from Dec 15, 2011, 23:46 UT to Dec 16, 2011, 00:16 UT.}
    \label{fig:remap_slits}
\end{figure}

\begin{figure}[htpb]
    \centering
    \includegraphics[width=1.0\textwidth]{figure5.png}
    \caption{Same as in Fig. \ref{fig:remap_slits} but for the outbound phase of the comet trajectory. The striae marked by blue lines are labelled as S4--S6. The animation of this figure is available (outbound.mp4). The nine seconds video covers the transit of Comet Lovejoy on Dec 16, from 00:40 to 01:28.}
    \label{fig:remap_slits2}
\end{figure}

The analysis of the TD maps can provide some information in the evolution of the oxygen ion emission. The signature of a stria in a TD map is in the majority of the cases pretty diffuse and extends along the positive direction of the vertical axis. We see a sharp boundary denoting the propagating front of the ions and a bright core moving more slowly.
In addition, the emission also slowly propagates in the negative direction of the distance axis because of dispersion effects on the moving ions. The emission in the TD maps for slits S4 and S5 is very narrow and straight, indicating that the ions are quickly transported along the magnetic field lines. The emission starts almost one minute after the comet transit and lasts for a shorter time with respect to the other striae because of the higher collision rate with coronal particles. Given a  time interval $\delta t = 2$ min and an apparent distance covered by the emission of $\Delta s \sim (20-25)\times10^3$ km, the slope of the emission in the TD maps for S4 and S5 can be associated with an average ion beam speed of 167-208 km s$^{-1}$. In the other cases, we also see some signatures coming from nearby structures, like a diffuse emission at the right side of the TD maps for the slits S2 and S6. In particular for S3, the shape of the stria signature has an inverted \lq\lq V\rq\rq-shape, which is the result of the merging of nearby striae, as it is found by inspecting the animation inbound.mp4.

\begin{figure}[htpb]
    \centering
    \begin{tabular}{c c}
        \includegraphics[width=0.5\textwidth]{S1_ni.png}  &
        \includegraphics[width=0.5\textwidth]{S2_ni.png}\\
        \includegraphics[width=0.5\textwidth]{S3_ni.png}  &
        \includegraphics[width=0.5\textwidth]{S4_ni.png}\\
        \includegraphics[width=0.5\textwidth]{S5_ni.png}  &
        \includegraphics[width=0.5\textwidth]{S6_ni.png}\\
    \end{tabular}
    \caption{Time distance maps relative to the slits S1--S6 marked in Fig. \ref{fig:remap_slits}. The position of the beam as a function of time obtained from Eq. \eqref{eq_beam} at time steps of 24 s are overplotted as red dots in the TD maps for slits S4 and S5. For details, see Sect. \ref{subsec:comp}.}
    \label{fig:tdmap_slits}
\end{figure}

\subsection{Comparison between observational and modeling profiles}
\label{subsec:comp}

By focusing on the emission signature, the intensity profile at 171 {\AA} as a function of distance at a given time (i.e., the intensity coming from a vertical line in the TD map) is compared with the squared density from Eq. \eqref{eq:eq_density_final} in Fig. \ref{fig:obs_mod_profiles_01}-\ref{fig:obs_mod_profiles_02}. The latter is integrated numerically via Simpson's rule and is computed over a spatial interval $[-5, 5]\times 10^4$ km with an integration step $\Delta x = 100$ km. The integration in time is performed in a time interval of 600 s spanning the comet transit with a time step $\Delta t =$ 12 or 24 s.

EUV intensity and ion beam density are not directly comparable quantities. The EUV intensity from a pixel at a given wavelength $I_\lambda$ is defined as the convolution of the response function of the EUV filter $R_\lambda$ with the differential emission measure integrated along the line-of-sight $h^\prime$ \citep{2004psci.book.....A,2012SoPh..275...41B}:
\begin{equation}
    I_\lambda = \int_0^\infty R_\lambda(T) DEM(T) dT,
\end{equation}
where the differential emission measure is defined as $DEM(T) = n^2(T, h') \frac{dh'}{dT}$ with $n$ being the free electron density of cometary origin, therefore proportional to the oxygen density \citep[Supplementary Material][]{Schrijver2012}. However, if we assume that oxygen ions are formed at a specific temperature value $T_0$ (see Table 1 of \citet{McCauley2013}, where the temperature peaks for oxygen ions based on the CHIANTI model under the hypothesis of equilibrium conditions are reported) and that the density is approximately constant through the stria column depth $h$, the DEM function can ideally be expressed in terms of a delta function $DEM(T) = n^2 \frac{dh'}{dT}\delta(T-T_0)$, hence:
\begin{equation}
    I_\lambda = \int_0^h R_\lambda(T_0) n^2(T_0) dh' = R_\lambda(T_0) n^2(T_0) \int_0^h dh' =  R_\lambda(T_0) h~n^2(T_0),
\end{equation}
with $h$ the column depth of the stria. Therefore, provided the column depth $h$ does not vary, under such assumptions, the intensity differs from the squared density only by the multiplicative factor $R_\lambda(T_0) h$. On the other hand, the computation of the theoretical intensity fluxes (in units of photons s$^{-1}$ or DN s$^{-1}$) would require that the response function $R_\lambda$ is not based on the ordinary coronal abundances but instead on those of the mixture of coronal and cometary plasma. We avoid this issue by subtracting a background level to the stria intensity profiles and normalising these to their maximum.

The observed intensities and squared density profiles are given as blue and red lines, respectively, in Fig. \ref{fig:obs_mod_profiles_01} for slits S1--S3, S6, and in Fig. \ref{fig:obs_mod_profiles_02} for slits S4--S5. The parameters used to define the computed density profiles are educated guesses, obtained by doing several manual trials until the red line does qualitatively fit the observed profiles. More specifically, we followed these steps:
\begin{itemize}
    \item given a set of starting guessed values for the parameters, we numerically integrate Eq. \eqref{eq_density} and overplotted the computed squared density against the intensity profile;
    \item we visually checked the overlap of the profiles, both in time and space;
    \item if the profiles did not match well, we proceeded by changing the value of one parameter, we re-computed the modelled density and compared to the observed intensity profile. If the profiles did not overlap again, we re-did the procedure;
    \item when finding the best-fitting squared density profile, we changed one parameter at a time to empirically understand its effect on the trend of the profile (e.g., peak height and position, steepness of the profile, etc.).
\end{itemize}
Since the model has a large number of parameters, a Markov-Chain Monte Carlo approach would be suitable for a more robust fit \citep{2021ApJS..252...11A}. We defer this to a future work. The value of the parameters that we determined are reported in each panel of Fig. \ref{fig:obs_mod_profiles_01} and \ref{fig:obs_mod_profiles_02} and also listed in Table \ref{tab:tab2}. The intensity profiles from each slit are given with a time interval of 24 s, except for those from the slits S4 and S5 where the evolution is quicker and we preferred to show it every 12 s.

The theoretical profiles shown in Fig. \ref{fig:obs_mod_profiles_01} are in good agreement with the observed ones for the given sets of parameters that we have determined. In the case of the intensity profiles from slits S4 and S5 (Fig. \ref{fig:obs_mod_profiles_02}), we were not able to fit well the observed intensity profiles for all the instants of time (dashed grey lines). The reasons might be different: e.g., misalignment of the slit with the stria; non-constancy of $\tau_{slow}$ because of non-negligible gravitational stratification effects; motion of the background coronal plasma due to blobs or MHD waves \citep{2021ApJ...909..202C}; the influence of plasma instabilities on the evolution of cometary plasma. Also, a varying initial speed of the ions, as the comet could be subject to some evolution  because of the solar radiation, might affect the observed intensity profiles. However, as the main reason we indicate the variable projection of the ion beam motion due to non-straight magnetic field lines. The region where S4 and S5 are located is possibly made of a system of magnetic field loops viewed mostly edge-on to the comet path and then bending and becoming more transverse with respect to the line-of-sight, as also suggested in \citet[]{Downs13} and \citet{Raymond2014}, while the striae for the other slits would be straight flux tubes. The beam motion for S4 and S5 would be inevitably affected by the curvature of the loops, and the apparent speed would be much smaller than the \lq\lq true\rq\rq one when the motion of the ion beam is almost parallel to the line-of-sight direction. For example, we notice that in the slits S4 and S5 the cloud of cometary ions did not move too much in space before getting visible. In fact, if we consider the time lag after the comet transit ($\Delta t \sim 50$ s, as reported in black in the intensity time series of Fig. \ref{fig:obs_mod_profiles_02}) and the location of the peak ($\Delta s \sim (2-4)\times10^3$ km) at its first appearance, the corresponding average beam speed would be of 40-80 km s$^{-1}$, which is in disagreement with those estimated from the slope of the bright feature in the TD maps (an acceleration of the ion beam could not be easily explained). On the other hand, we could expect that, as the ion beam descends along the loop, it progressively outlines the loop leg, which is less curved. Therefore, to mitigate the effect of the loop curvature and to avoid modelling the early phase of the ion beam propagation, when fitting the intensity profiles from S4 and S5, we considered a temporal shift and took as a reference a time instant before the appearance of the peak in the observed intensity profiles. The shifted time intervals are shown in red in Fig. \ref{fig:obs_mod_profiles_02} and labelled as $t^\star$. For these specific cases, the quantity $u_0$ will continue to be the ion beam injection speed, but no longer defined at the time of the comet transit but at the instant of time that we took as a reference. The computed and re-defined profiles are shown in red against intensity profiles (in blue) and the former profiles computed with respect to the comet time transit (dashed grey lines). We also report the value of the physical parameters for both theoretical profiles (in squared brackets those for the dashed grey lines). In general, there is an improvement in the overlap between the model and the observations: the injection beam $u_0$ is of the same order of the average speed inferred from the TD maps; the peak of the theoretical profile tends to overlap with that from the observations until $t^\star\approx 60$ s, later a mismatch in space is found probably caused by the residual curvature of the loop, whose effect was not fully removed. However, the position of the beam front, as computed by Eq. \eqref{eq_beam} and depending on $u_0$ and $\tau_{slow}$, results to be in a good agreement with the stria signature in the TD maps (Fig. \ref{fig:tdmap_slits}). Despite the above discrepancies, we provisionally consider that the values obtained for $\tau_{slow}$ and $\tau_D$ are appropriate, as a first estimate, for the striae under study.

\begin{table}[htpb]
    \centering
    \begin{tabular}{l c c c | c c c c c | c c c }
    \hline
    \hline
    Slit & $t_c$ & $r_c$ & $v_c$ & $u_0$       & $t_0$ & $\sigma_{t_0}$ &  $\tau_{slow}$ & $\tau_{D}$  & $n_{\tau_{slow}}$ & $n_{\tau_D}$ & $n_e \pm \Delta n_e$   \\
        & hh:mm:ss & [R$_\odot$] & [km s$^{-1}$]    &  [km s$^{-1}$]  &  [s]  & [s]  & [s] & [s] & [$10^7$ cm$^{-3}$] & [$10^7$ cm$^{-3}$] & [$10^7$ cm$^{-3}$]\\
    \hline
        S1              & 23:53:57 & 1.57 & 493 &  60 &  90 &  80 & 400 &  40 & 3.6 & 6.4 & $5.0 \pm 1.4$   \\
        S2              & 23:56:00 & 1.52 & 500 &  70 &  90 &  80 & 250 &  60 & 5.8 & 4.3 & $5.1 \pm 0.8$ \\
        S3              & 23:57:14 & 1.50 & 504 &  80 & 120 &  80 & 400 &  50 & 3.7 & 5.1 & $4.4 \pm 0.7$ \\
        S4$^\star$ & 00:44:25 & 1.38 & 525 & 250 &  30 &  30 & 150 &  30 &10.7 & 8.6 & $9.6 \pm 1.1$ \\
        S5$^\star$ & 00:45:45 & 1.40 & 521 &  200 &  20 &  20 & 200 &  50 & 7.9 & 5.1 & $ 6.5 \pm 1.4$ \\
        S6             & 00:50:58 & 1.50 & 504 &  50 &  80 & 200 & 300 & 100 & 4.9 & 2.6 & $3.8 \pm 1.2$ \\
    \hline
    \hline
    \end{tabular}
    \caption{Values of the parameters used to reproduce the intensity of the striae (see text for further details). The two inferred coronal electron densities, namely $n_{\tau_{slow}}$ from Eq. \eqref{eq:tau_slow}, and $n_{\tau_D}$ from Eq. \eqref{eq:tau_d}, are also shown with their combined average. The symbol $^\star$ indicates those striae whose intensity profiles are fitted in a less satisfactory way than the others, see Sect. \ref{subsec:comp}.}
    \label{tab:tab2}
\end{table}

\begin{figure}[htpb]
    \centering
    \begin{tabular}{c c}
        \includegraphics[width=0.5\textwidth]{int_prof_fit_S1_final.png} &
        \includegraphics[width=0.5\textwidth]{int_prof_fit_S2_final.png} \\
        \includegraphics[width=0.5\textwidth]{int_prof_fit_S3_final.png} &
        \includegraphics[width=0.5\textwidth]{int_prof_fit_S6_final.png} \\
    \end{tabular}
    \caption{Intensity profiles for the slits S1--S3 and S6 recorded with SDO/AIA (blue lines) and compared with the squared density profiles obtained from the modeling (red lines). }
    \label{fig:obs_mod_profiles_01}
\end{figure}

\begin{figure}[htpb]
    \centering
    \begin{tabular}{c c}
        \includegraphics[width=0.5\textwidth]{int_prof_fit_S4_final.png} &
        \includegraphics[width=0.5\textwidth]{int_prof_fit_S5_final.png} \\
    \end{tabular}
    \caption{Intensity profiles for the slits S4 and S5 as blue lines vs. squared density profiles obtained from the modeling (red line). For the density profiles we applied a temporal shift (the values of $t^\star$ in red) to better fit the rise of the intensity peak. The density profiles referred to the time of the comet transit (the values of $t$ in black) are also shown as dashed gray lines. Different values of the parameters for these profiles as given inside square brackets. The vertical dotted black line represents the position of the beam front, computed from Eq. \eqref{eq_beam} and analogous to the red points shown in the TD maps for slits S4 and S5.}
    \label{fig:obs_mod_profiles_02}
\end{figure}

\subsection{Determination of the electron density in the striae}

Once the computed profiles fit the observed ones, we used the values of $\tau_{slow}$ and $\tau_D$ to infer the electron density in the striae by using Eqs. \eqref{eq:tau_slow} and \eqref{eq:tau_d}.
The expression of $\tau_{slow}$ depends on the injection velocity $U$ that we have assumed equal to the corresponding value $v_c$ listed in the Table \ref{tab:tab2}. The dispersion time $\tau_D$ depends on the random velocity $v_\mathrm{ran}$ that we estimated be to be 150 km s$^{-1}$ for all the analysed striae. Therefore, we provide two distinct estimates for the electron density, $n_{\tau_{\rm slow}}$ and $n_{\tau_D}$, which are also reported in Table \ref{tab:tab2}.
In Fig. \ref{fig:tauslow_vs_ne}-left we show the dependence of $\tau_{slow}$ (solid blue line) and $\tau_D$ (dotted blue line) as a function of $n_e$. The solid line for $\tau_{slow}$ is obtained for a typical speed of the comet $U=500$ km s$^{-1}$. The data points are given as red dots for all the analysed slits, except for the slits S4 and S5, which are given as green triangles because the fit is less satisfactory for these two striae.

The obtained estimates of density $n_{\tau_{\rm slow}}$ and $n_{\tau_D}$ are different but of the same order of magnitude. To define a single value of the coronal electron density for each  stria, we considered the average between these two estimates, i.e., $n_e = 0.5(n_{\tau_{\rm slow}} + n_{\tau_D})$ with an uncertainty simply given as the absolute semi-difference between $n_{\tau_{\rm slow}}$ and $n_{\tau_D}$  , i.e., $\Delta n_e = 0.5 | n_{\tau_{\rm slow}} - n_{\tau_D}|$. The right panel of Fig. \ref{fig:tauslow_vs_ne} shows the values of $n_e$ with the associated error bars as a function of the radial distance $r_c$ where each striae is formed. The data points are compared with a hydrostatic density profile $n(r) = n_0 \exp\left[-(r-R_\odot)/H\right]$, with  $H$ the pressure scale height defined as $H=2 k_B T_e/\mu m_p g_\odot$, with $k_B$ the Boltzmann constant, $\mu$ the mean molecular weight, and $g_\odot$ the solar gravity acceleration. We have considered $g_\odot= 274\times10^4$ cm s$^{-2}$, constant and not varying with altitude since the height of the analysed striae is $<1.5$R$_\odot$ \citep[this is the plane-parallel hydrostatic solution as presented in][]{Zucca2014}. We plotted different profiles for different values of $n_0$, the initial value of density at the solar surface. The data points tend to cluster along the lines for $n_0 = [5, 10] \times 10^{9}$ cm$^{-3}$.

\begin{figure}[htpb]
    \centering
    \begin{tabular}{c c}
        \includegraphics[width=0.5\textwidth]{tau_slow_vs_ne.png} &
        \includegraphics[width= 0.5\textwidth]{ne_vs_distance.png}
    \end{tabular}
    \caption{Left: graph showing the trend of $\tau_{slow}$ (left axis, solid line) and $\tau_D$ (right axis, dotted line) as a function of the electron density $n_e$. The solid blue line for $\tau_{slow}$ is computed with a speed $U=$500 km s$^{-1}$ (the comet speed), while the dotted one for $\tau_D$ with $v_\mathrm{ran} = 150$ km s$^{-1}$ (the thermal speed). The two data points as green triangles refer to the slits S4 and S5. Right: electron density in logarithmic units as a function of the radial distance in $R_\odot$. The data points as green triangles refer to slits S4 and S5. The data points are compared with a hydrostatic density model for different values of the density at the solar surface $n_0$ and with $T=$1.5 MK.}
    \label{fig:tauslow_vs_ne}
\end{figure}

\section{Discussion and conclusions} \label{sec:disc}

In this paper we present a new diagnostic method to estimate the electron density in the solar corona, at heights so low as those traveled by the sungrazing Comet C/2011 W3 (Lovejoy), which was observed in December 2011 \citep{Downs13}. In-situ measurements of the density in the solar corona at heights of hundred thousands of kilometers above the photosphere are currently not possible. In addition, measurements from remote-sensing instruments are affected by large uncertainties due to integration of emission at a certain wavelength along the line-of-sight. The method demonstrated here is based on the EUV emission of oxygen ions of cometary origin, which propagate along the local magnetic field and form the intriguing structures known as striae. Comet Lovejoy is the only comet that was observed to cross the solar corona and to survive the perihelion transit as seen from SDO/AIA \citep{Downs13} by leaving a trail of many and in some cases long-lived striae.
The length and the spreading of striae left by Comet Lovejoy and observed in the 171 channel are related to the collision times for the slowing down of a suprathermal beam and for the diffusive spreading of suprathermal ions. These collision times directly depend on the ambient coronal density, so that a determination of them readily gives a density estimate (see Eqs. \eqref{eq:tau_slow}-\eqref{eq:tau_d}). The fitting procedure of the intensity profiles of the striae allow to determine the best values of the slowing down time $\tau_{slow}$ and the dispersion time $\tau_D$. On the other hand, a number of simplifying assumptions, like constant ambient temperature, constant ambient density, straight magnetic field lines, steady release of the ions, etc., is needed in order to extract these first results. Also, a careful data handling is necessary, since some misalignment is present between images in the sequence captured by SDO/AIA.

The electron density was computed numerically with the use of our model and compared qualitatively with the observed intensity profile. We did several trials in order to get profiles as close as possible to the observed ones, by varying one parameter at a time. The matching between observations and model is mainly evaluated based on the position and height of the intensity peak, and the width of the tails.
Therefore, we have shown that such an approach is useful for understanding the density structure of the solar corona with a local diagnostics once $\tau_{slow}$ and $\tau_D$ are evaluated.

In spite of some uncertainty in the obtained values of the electron density, which are in the range of $10^7-10^8$ cm$^{-3}$, we can compare them with other estimates from the literature.
\citet{McCauley2013} provides an estimate of density by considering the offset in space between the leading edge of the emission observed simultaneously in different EUV filters (which again outlines different states of ionisation for oxygen, e.g., 304 \AA~for O$^{2+}$ and 131~\AA~for O$^{5+}$) and the ionisation rate coefficients, which are linked by Eq. 2 reported in their work. By analysing the EUV emission observed around 00:46:12 UT on December 16, hence in a region of the corona included between our slits S4 and S5, they found a density of $\sim1.4 \times 10^8$, which is \sout{very} close to our values for these slits.
\citet{Raymond2014} have also given some estimates of the local electron density for the same region of interest with two different approaches: the former based on the ratio between the ionisation time of the cometary hydrogen and oxygen atoms and the typical crossing time of a stria by the comet, the latter by taking into account the emission measure, the filling factor and a typical coronal length scale observed in the striae. They give an upper limit value for the inter-striae regions of $2.7\times10^6$ cm$^{-3}$, while within a stria the lower and upper limit are evaluated as $1.7\times10^7 - 1.4\times10^8$ cm$^{-3}$, in reasonable agreement with our results.
On the other hand, our values of $n_e$ are somewhat larger than those found at the same coronal heights by \citet{Zucca2014} for both active regions and the quiet sun (see their Figure 10). Those density estimates were obtained by interpolating the densities obtained at lower altitudes by SDO/AIA and at higher altitudes by SoHO/LASCO by means of the emission measure, which is integrated along the line of sight. Therefore, those coronal densities are average values while our estimates are local values. The fact that the local values are somewhat larger than the average values agrees with the idea that coronal density is strongly spatially structured \citep[for the physical causes of such a structuring see the discussion in][]{Raymond2014}, and that the observation of striae is due to the fact that the comet is crossing regions of quickly changing density, with denser regions giving rise to larger erosion of cometary material and therefore brighter UV emission. Such a density fine structuring could also be attributed to the bimodal structure of the lower solar wind detected higher up from 6 to 21 solar radii \citep{2018PhRvL.121g5101C}.

The determination of the coronal electron density that we propose is complementary to differential emission measure analysis techniques that are widely used \citep{2012A&A...539A.146H,2015ApJ...807..143C} but not applicable to the case of cometary plasma because the condition of ionisation equilibrium is not satisfied. Moreover, it is crucial in the context of coronal seismology \citep{2020ARA&A..58..441N}. In fact, the striae left by the comet were not static features but exhibited an apparent transverse motion, perhaps an evidence of propagating kink waves \citep{2021SSRv..217...73N} in the flux tubes outlined by the striae. The transverse motion of the striae is evident in the region that encompasses the slits S2 and S3 during the inbound transit of the comet, and the region around slit S6 during the outbound phase (see the animation anim.m4v of Fig. \ref{fig:remap_slits}). Such a prospect opens a further possibility for the inference of the coronal magnetic field in the low corona by MHD seismology.

The inhomogeneity of the plasma density revealed by the cometary striae could be due to the different densities in different magnetic flux tubes linked to solar granulation cells and small scale reconnection, which may inject different amounts of plasma in adjacent flux tubes through spicules or jets \citep{2009SoPh..259...87N, 2010AnGeo..28..687N}. These density variations can also be related to the density fine structures seen in solar eclipses images acquired from the ground, in particular in the polar regions \citep[e.g., see ][]{2009ApJ...702.1297P,2014ApJ...785...14D}. It is notable that the density structures seen in white light images have low contrast because of the line-of-sight integration, but the brightness contrast along the comet Lovejoy path reported by \citet{Raymond2014} suggests that the density ratio between adjacent flux tubes is of order six or more. Our study is consistent with those density ratios, and this gives interesting clues to the understanding of pressure balance in the low beta corona and to the dispersion of MHD waves propagating through such inhomogeneities \citep{2013A&A...549A..54M,2014A&A...569A..12N,2020ARA&A..58..441N}. Furthermore, the density fine structuring of the solar corona could also be studied with the upcoming observations of Solar Orbiter/Metis in white light and in the Lyman-$\alpha$ line \citep{2020A&A...642A..10A}, with the Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun (ASPIICS) on board the Project for On-Board Autonomy (PROBA-3) \citep{2021A&A...652A...4S}, and possibly be related to in-situ measurements with Parker Solar Probe \citep{2019Natur.576..228K,2021ApJ...920L..14T}.

The model that we presented here explores the role of collisions in the diffusion of cometary oxygen ions and in the slowing down of the ion beam. As already mentioned, other physical factors might be at work in the evolution of cometary ions along the coronal flux tubes. For example, the diffusion along the field could also be affected by turbulence (e.g., whistler turbulence or Langmuir turbulence). Furthermore, in this work we did not investigate the influence of the coronal density on the oxygen lifetime $\tau_L$ (where $\tau_L=(n_e q_i)^{-1}$, with $q_i$ the ionisation rate), which was kept as a fixed parameter in our analysis. It would be also interesting to apply this analysis to striae observed in the other EUV channels of SDO/AIA, in order to better constrain the density values of the solar corona. We will study all these aspects in follow-up works.
\\
\\
\\

Data are courtesy of the SDO/AIA team. G.N. acknowledges support from the \lq\lq Rita Levi Montalcini 2017\rq\rq fellowship contract funded by the Italian Ministry of University and Research for the project {\it \lq\lq Probing the heliospheric and near-Sun environments with comets\rq\rq}. V.M.N. acknowledges support from the STFC Consolidated Grant ST/T000252/1. Work of MD was supported by the Grant Agency of the Brno University of Technology (grant FSI-S14-2290). We thank the referee for his suggestions, comments and careful reading of our work.

\subsubsection*{#1}}

\pagestyle{headings}
\markright{Reference sheet: \texttt{natbib}}

\usepackage{shortvrb}
\MakeShortVerb{\|}

\begin{document}
\thispagestyle{plain}

\newcommand{\textsc{Bib}\TeX}{\textsc{Bib}\TeX}
\newcommand{\texttt{#1}\def\filedate{#2}\def\fileversion{#3}}}{\texttt{#1}\def\filedate{#2}\def\fileversion{#3}}}
\begin{center}{\bfseries\Large
    Reference sheet for \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ usage}\\
    \large(Describing version \fileversion\ from \filedate)
\end{center}

\begin{quote}\slshape
For a more detailed description of the \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package, \LaTeX\ the
source file \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\texttt{.dtx}.
\end{quote}
\head{Overview}
The \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package is a reimplementation of the \LaTeX\ |\cite| command,
to work with both author--year and numerical citations. It is compatible with
the standard bibliographic style files, such as \texttt{plain.bst}, as well as
with those for \texttt{harvard}, \texttt{apalike}, \texttt{chicago},
\texttt{astron}, \texttt{authordate}, and of course \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}.

\head{Loading}
Load with |\usepackage[|\emph{options}|]{|\texttt{#1}\def\filedate{#2}\def\fileversion{#3}}|}|. See list of
\emph{options} at the end.

\head{Replacement bibliography styles}
I provide three new \texttt{.bst} files to replace the standard \LaTeX\
numerical ones:
\begin{quote}\ttfamily
 plainnat.bst \qquad abbrvnat.bst \qquad unsrtnat.bst
\end{quote}
\head{Basic commands}
The \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package has two basic citation commands, |\citet| and
|\citep| for \emph{textual} and \emph{parenthetical} citations, respectively.
There also exist the starred versions |\citet*| and |\citep*| that print
the full author list, and not just the abbreviated one.
All of these may take one or two optional arguments to add some text before
and after the citation.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citet{jon90}| & Jones et al. (1990)\\
  |\citet[chap.~2]{jon90}| & Jones et al. (1990, chap.~2)\\[0.5ex]
  |\citep{jon90}| & (Jones et al., 1990)\\
  |\citep[chap.~2]{jon90}| & (Jones et al., 1990, chap.~2)\\
  |\citep[see][]{jon90}| & (see Jones et al., 1990)\\
  |\citep[see][chap.~2]{jon90}| & (see Jones et al., 1990, chap.~2)\\[0.5ex]
  |\citet*{jon90}| & Jones, Baker, and Williams (1990)\\
  |\citep*{jon90}| & (Jones, Baker, and Williams, 1990)
\end{tabular}
\end{quote}
\head{Multiple citations}
Multiple citations may be made by including more than one
citation key in the |\cite| command argument.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citet{jon90,jam91}| & Jones et al. (1990); James et al. (1991)\\
  |\citep{jon90,jam91}| & (Jones et al., 1990; James et al. 1991)\\
  |\citep{jon90,jon91}| & (Jones et al., 1990, 1991)\\
  |\citep{jon90a,jon90b}| & (Jones et al., 1990a,b)
\end{tabular}
\end{quote}

\head{Numerical mode}
These examples are for author--year citation mode. In numerical mode, the
results are different.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citet{jon90}| & Jones et al. [21]\\
  |\citet[chap.~2]{jon90}| & Jones et al. [21, chap.~2]\\[0.5ex]
  |\citep{jon90}| & [21]\\
  |\citep[chap.~2]{jon90}| & [21, chap.~2]\\
  |\citep[see][]{jon90}| & [see 21]\\
  |\citep[see][chap.~2]{jon90}| & [see 21, chap.~2]\\[0.5ex]
  |\citep{jon90a,jon90b}| & [21, 32]
\end{tabular}
\end{quote}
\head{Suppressed parentheses}
As an alternative form of citation, |\citealt| is the same as |\citet| but
\emph{without parentheses}. Similarly, |\citealp| is |\citep| without
parentheses. Multiple references, notes, and the starred variants
also exist.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citealt{jon90}| & Jones et al.\ 1990\\
  |\citealt*{jon90}| & Jones, Baker, and Williams 1990\\
  |\citealp{jon90}| & Jones et al., 1990\\
  |\citealp*{jon90}| & Jones, Baker, and Williams, 1990\\
  |\citealp{jon90,jam91}| & Jones et al., 1990; James et al., 1991\\
  |\citealp[pg.~32]{jon90}| & Jones et al., 1990, pg.~32\\
  |\citetext{priv.\ comm.}| & (priv.\ comm.)
\end{tabular}
\end{quote}
The |\citetext| command
allows arbitrary text to be placed in the current citation parentheses.
This may be used in combination with |\citealp|.
\head{Partial citations}
In author--year schemes, it is sometimes desirable to be able to refer to
the authors without the year, or vice versa. This is provided with the
extra commands
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citeauthor{jon90}| & Jones et al.\\
  |\citeauthor*{jon90}| & Jones, Baker, and Williams\\
  |\citeyear{jon90}|   & 1990\\
  |\citeyearpar{jon90}| & (1990)
\end{tabular}
\end{quote}
\head{Forcing upper cased names}
If the first author's name contains a \textsl{von} part, such as ``della
Robbia'', then |\citet{dRob98}| produces ``della Robbia (1998)'', even at the
beginning of a sentence. One can force the first letter to be in upper case
with the command |\Citet| instead. Other upper case commands also exist.
\begin{quote}
\begin{tabular}{rl@{\quad$\Rightarrow$\quad}l}
  when & |\citet{dRob98}| & della Robbia (1998) \\
  then & |\Citet{dRob98}| & Della Robbia (1998) \\
     &   |\Citep{dRob98}| & (Della Robbia, 1998) \\
     &   |\Citealt{dRob98}| & Della Robbia 1998 \\
     &   |\Citealp{dRob98}| & Della Robbia, 1998 \\
     &   |\Citeauthor{dRob98}| & Della Robbia
\end{tabular}
\end{quote}
These commands also exist in starred versions for full author names.

\head{Citation aliasing}
Sometimes one wants to refer to a reference with a special designation,
rather than by the authors, i.e. as Paper~I, Paper~II. Such aliases can be
defined and used, textual and/or parenthetical with:
\begin{quote}
\begin{tabular}{lcl}
  |\defcitealias{jon90}{Paper~I}|\\
  |\citetalias{jon90}| & $\Rightarrow$ & Paper~I\\
  |\citepalias{jon90}| & $\Rightarrow$ & (Paper~I)
\end{tabular}
\end{quote}
These citation commands function much like |\citet| and |\citep|: they may
take multiple keys in the argument, may contain notes, and are marked as
hyperlinks.
\head{Selecting citation style and punctuation}
Use the command |\bibpunct| with one optional and 6 mandatory arguments:
\begin{enumerate}
\item the opening bracket symbol, default = (
\item the closing bracket symbol, default = )
\item the punctuation between multiple citations, default = ;
\item the letter `n' for numerical style, or `s' for numerical superscript
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\item the punctuation that comes between the author names and the year
\item the punctuation that comes between years or numbers when common author
      lists are suppressed (default = ,);
\end{enumerate}

The optional argument is the character preceding a post-note, default is a
comma plus space. In redefining this character, one must include a space if
one is wanted.

Example~1, |\bibpunct{[}{]}{,}{a}{}{;}| changes the output of
\begin{quote}
  |\citep{jon90,jon91,jam92}|
\end{quote}
into [Jones et al. 1990; 1991, James et al. 1992].

Example~2, |\bibpunct[; ]{(}{)}{,}{a}{}{;}| changes the output of
\begin{quote}
  |\citep[and references therein]{jon90}|
\end{quote}
into (Jones et al. 1990; and references therein).

\head{Other formatting options}
Redefine |\bibsection| to the desired sectioning command for introducing
the list of references. This is normally |\section*| or |\chapter*|.

Define |\bibpreamble| to be any text that is to be printed after the heading but
before the actual list of references.

Define |\bibfont| to be a font declaration, e.g.\ |\small| to apply to
the list of references.

Define |\citenumfont| to be a font declaration or command like |\itshape|
or |\textit|.

Redefine |\bibnumfmt| as a command with an argument to format the numbers in
the list of references. The default definition is |[#1]|.

The indentation after the first line of each reference is given by
|\bibhang|; change this with the |\setlength| command.

The vertical spacing between references is set by |\bibsep|; change this with
the |\setlength| command.

\head{Automatic indexing of citations}
If one wishes to have the citations entered in the \texttt{.idx} indexing
file, it is only necessary to issue |\citeindextrue| at any point in the
document. All following |\cite| commands, of all variations, then insert
the corresponding entry to that file. With |\citeindexfalse|, these
entries will no longer be made.

\head{Use with \texttt{chapterbib} package}

The \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package is compatible with the \texttt{chapterbib} package
which makes it possible to have several bibliographies in one document.

The package makes use of the |\include| command, and each |\include|d file
has its own bibliography.

The order in which the \texttt{chapterbib} and \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ packages are loaded
is unimportant.

The \texttt{chapterbib} package provides an option \texttt{sectionbib}
that puts the bibliography in a |\section*| instead of |\chapter*|,
something that makes sense if there is a bibliography in each chapter.
This option will not work when \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ is also loaded; instead, add
the option to \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}.

Every |\include|d file must contain its own
|\bibliography| command where the bibliography is to appear. The database
files listed as arguments to this command can be different in each file,
of course. However, what is not so obvious, is that each file must also
contain a |\bibliographystyle| command, \emph{preferably with the same
style  argument}.
\head{Sorting and compressing citations}
Do not use the \texttt{cite} package with \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}; rather use one of the
options \texttt{sort} or \texttt{sort\&compress}.

These also work with author--year citations, making multiple citations appear
in their order in the reference list.

\head{Long author list on first citation}
Use option \texttt{longnamesfirst} to have first citation automatically give
the full list of authors.

Suppress this for certain citations with |\shortcites{|\emph{key-list}|}|,
given before the first citation.

\head{Local configuration}
Any local recoding or definitions can be put in \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\texttt{.cfg} which
is read in after the main package file.

\head{Options that can be added to \texttt{\char`\\ usepackage}}
\begin{description}
\item[\ttfamily round] (default) for round parentheses;
\item[\ttfamily square] for square brackets;
\item[\ttfamily curly] for curly braces;
\item[\ttfamily angle] for angle brackets;
\item[\ttfamily colon] (default) to separate multiple citations with
     colons;
\item[\ttfamily comma] to use commas as separaters;
\item[\ttfamily authoryear] (default) for author--year citations;
\item[\ttfamily numbers] for numerical citations;
\item[\ttfamily super] for superscripted numerical citations, as in
     \textsl{Nature};
\item[\ttfamily sort] orders multiple citations into the sequence in
     which they appear in the list of references;
\item[\ttfamily sort\&compress] as \texttt{sort} but in addition multiple
     numerical citations are compressed if possible (as 3--6, 15);
\item[\ttfamily longnamesfirst] makes the first citation of any reference
     the equivalent of the starred variant (full author list) and subsequent
     citations normal (abbreviated list);
\item[\ttfamily sectionbib] redefines |\thebibliography| to issue
     |\section*| instead of |\chapter*|; valid only for classes with a
     |\chapter| command; to be used with the \texttt{chapterbib} package;
\item[\ttfamily nonamebreak] keeps all the authors' names in a citation on
     one line; causes overfull hboxes but helps with some \texttt{hyperref}
     problems.
\end{description}
\end{document}

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Mark By: Mark
Lincoln, Subdeanery
Precentory, now subdeanery and offices. C13 and C14, with C17 additions. Remodelled and extended 1827. Refronted 1873 by J L Pearson. A Roman hypocaust and mosaic pavement were found on the site in the C18, and remain in situ. Dressed stone and brick, with stucco east front, ashlar dressings and plain tile roofs, with 4 gable and single ridge and side wall stacks. EXTERIOR: sill band, 2 string courses, eaves band, coped parapet and gables to north and east fronts. 2 and 3 storeys, 3 bays. L-plan. North front has steps in the return angle to the right, with a moulded four-centred arched doorway with hoodmould, sidelights and overlight. Above it, a 4-light stone mullioned cross casement. To the left, a square bay window, 2 storeys, with a similar 4-light window on each floor. East front has a wooden doorcase with cornice and recessed 6-panel door, flanked to right by a glazing bar sash. Above, 3 glazing bar sashes. To the left, a square stair tower with parapet, with single light windows on the lower floors and a cross casement above. South side has two fronts, 2 and 3 storeys, 3 bays, with glazing bar casements. INTERIOR No.18A has partly panelled entrance hall, late C17, with wooden fireplace and overmantel and moulded beams. First floor room with similar fielded panelling. In the basement a section of Roman tessellated pavement approx. 1 x 1.5m, and a medieval cistern. Towards the rear, a Roman hypocaust reached by a stone winder stair in a stone lined round arched stairwell. At the foot of the stairs, a segment arched recess opposite a round arched brick firehole. The hypocaust, approx. 10m x 5m, has square brick columns carrying a terracotta floor. EH Listing


NASA's new vision to return humans to the Moon is the next practical step in expanding human habitation beyond Earth. As the Habitation 2006 Conference website states: "new knowledge and new technologies are required." Along with the development of new habitation systems, an important consideration is how to transport these heavy structures cheaply to the Moon? We propose the use of ultra-low-energy orbits in the Interplanetary Superhighway as an economical and effective means to deliver cargo to the Moon. This approach not only reduces the propulsion cost, but also provides enormous flexibility and robustness to the mission architecture.


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Good Samaritan now regrets chasing thieves who broke into woman's car
Greg Mobley said he regrets his decision to chase after two suspects who stole a woman's purse. (Photo: WSBTV.com)
By Carl Willis, WSBTV.com
A good Samaritan who tried to chase down robbers says he regrets his decision.
"I was in the wrong, and I would, I would, never do it again." Greg Mobley told Channel 2's Carl Willis.
Mobley pulled into an Exxon gas station at Bolton and Marietta roads on Wednesday when he heard a woman screaming for help. He decided to act.
"It's a spur of the moment thing and you don't realize it, until they're looking at you in your eyes and they're asking for help from anybody," he said.
On Thursday, Mobley met Willis at the scene and described how he used his truck to try to stop the thieves. They had just shattered the victim's window and stolen her purse.
Mobley said he tried to cut them off, or possibly clip their car, but he missed when they swerved around.
"They were quick and they weren't afraid of much. And they just didn't seem like they valued even their life," he said.
He said traffic was blocked by a MARTA bus, but the thieves continued to maneuver west on Bolton.
Mobley said he only pulled back when they ratcheted up the threat to him and everyone around.
"One of them did stick a gun out the window to let me know that they had a gun. But there was a time when I could have pinned them under that MARTA bus."
Ultimately, he decided he didn't want to take the pursuit too far. Mobley told Willis he even regrets chasing after the young thieves.
"I just went and sat by myself for a 15-20 minutes and I just cried," Mobley said. "I mean it was sad; I could have really hurt (them). It could have been a really horrible thing. It won't be me again. I won't ever do that again."
Carl Willis, WSBTV.com


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Recommind Adds eDiscovery to MindServer
by Paula J. Hane
Recommind (www.recommind.com) has launched a new version of its MindServer platform, which includes new eDiscovery functionality that enables enterprises to quickly and easily locate electronically stored information that must be preserved—and produced—for ongoing or anticipated litigation. The company said the new MindServer 5.0 also adds improved APIs (application program interfaces) to make the platform more friendly for OEM partners and offers significant performance improvements. Recommind has historically been a leader in the legal marketplace, but, with the debut of the capabilities in this new version, it expects to accelerate adoption within other information-intensive vertical markets, including retail, pharmaceuticals, media, and healthcare.
The MindServer 5.0 enterprise search and categorization platform automatically organizes, manages, and distributes large volumes of information from multiple sources, including documents, presentations, emails, Web pages, newsfeeds, and data from other applications. It features a conceptual search capability so that users can retrieve relevant documents that don't contain the exact keywords used for a search.
The debut of the new eDiscovery component in MindServer 5.0 was driven by the new Federal Rules of Civil Procedure (FRCP), which went into effect on Dec. 1, 2006. U.S. companies now have an obligation to preserve relevant information (documents, email, etc.) when litigation commences or can be reasonably anticipated. Failure to preserve and provide such potential evidence can result in fines, court sanctions, discovery penalties, and adverse judgments. (Morgan Stanley was fined $15 million in May 2006 when it failed to provide email messages related to investigations.) Forrester Research expects the eDiscovery technology market to grow from $1.5 billion in 2006 to $4.9 billion by 2011 (note: this does not include consulting or forensics).
Recommind claims that MindServer 5.0 is unique among enterprise search solutions in its ability to quickly identify and find potentially relevant and responsive enterprise information that must be preserved as part of a litigation hold, a requirement of any legal proceeding. In many enterprise environments, the MindServer platform itself can lock down any document or other piece of information returned in a search query. Otherwise, MindServer 5.0 is able to pass the results set from any query to a separate application, such as a content management system or a database, for immediate litigation hold lockdown. The company also said that MindServer 5.0 supports multiselection filters within the user interface, a prerequisite for the highly comprehensive and detailed searches needed for effective litigation hold.
Browning Marean, partner at DLA Piper US LLP, said: "Recent revisions to the Federal Rules of Civil Procedure (FRCP) specifically address Electronically Stored Information (ESI), what it is and how it must be produced during litigation. Before large enterprises can even attempt to produce such information, however, they must identify and preserve it, which can be extremely difficult and time-consuming under the best of circumstances. The litigation hold feature in MindServer 5.0 is an elegant solution to this vexing problem."
Craig Carpenter, Recommind's vice president of marketing, said that manual solutions to the document-preservation needs of large enterprises can be too slow and not sufficiently accurate. Solutions from email-archiving vendors don't cover other critical components, such as file servers, databases, CRM systems, and Web servers. Outsourcing to litigation-support firms is expensive and can be disruptive. Carpenter explained that an ideal solution to eDiscovery and litigation hold would be easy to use, accurate and relevant, and would overlay legacy databases and applications—all features offered by MindServer 5.0. He also said that Recommind's customers want an automated system that learns on-the-fly (for example, that "poison pill" relates to takeovers) and one that scales and maintains performance. "The more dynamic the environment, the greater need there is for Recommind."
Companies will definitely have to be more proactive about e-document preservation, no matter what solution they choose. Industry experts seem to feel that the new rules will boost the demand for all types of tracking and archiving solutions. Some vendors are calling it an opportunity.
Analyst Michael Dortch, director of IT infrastructure management strategies at Robert Frances Group, said that the average large corporation probably faces about 50-80 serious lawsuits at any given time. He said that companies with lots of rapidly changing information and that are highly regulated will see the attraction of this type of software solution—when failure to comply can mean "dollars on the table in significant amounts." He thinks that "2007 will be a tipping point," as enterprises respond to FRCP. Dortch also said that he expects to see more alliances and partnerships among enterprise-solutions vendors, as well as more M&A activity. Recommind will be in a good position, he said, since the company "understands the business side of the problems, not just the technology."
Recommind's customers include the U.S. National Library of Medicine, DuPont, the Australian government, and Bertelsmann AG. Founded in 2000 by researchers from the University of California-Berkeley, MIT, and Brown University, Recommind is privately held and reports that it is profitable. The company is headquartered in San Francisco and has offices in New York, London, and Bonn, Germany.
For more information on Recommind and its technology, see the NewsBreak from May 22, 2006, about the launch of MindServer 4.2 (http://newsbreaks.infotoday.com/nbReader.asp?ArticleId=15785).
For more information on FRCP, see the cover article by Jonathan Spira in the January 2007 issue of KMWorld, "Electronic content—a federal case" (www.kmworld.com/Articles/ReadArticle.aspx?ArticleID=18860), and an article in InformationWeek by Rick Whiting, "New Data-Archiving Rules Impact IT Managers" (www.informationweek.com/management/showArticle.jhtml?articleID=196800629&subSection=Global).
Also see the information about FRCP posted by LexisNexis at https://www.lexisnexis.com/applieddiscovery/lawLibrary/courtRules.asp.
Material regarding the amendments to FRCP is available on the U.S. Court's Federal Rulemaking site at www.uscourts.gov/rules/congress0406.html.
Paula J. Hane is a freelance writer and editor covering the library and information industries. She was formerly Information Today, Inc.'s news bureau chief and editor of NewsBreaks.
5/9/2011 Recommind Forms Strategic Alliance With LexisNexis for Hosted eDiscovery


These requirements might seem stringent and difficult to produce, but an easy way to make it happen is to work with FRS Pros. We can help you maintain a secure network for all of your organization's sensitive information, including card information. To learn more, reach out to us at 561-795-2000.